Catastrophic Cooling in Superwinds. III. Non-equilibrium Photoionization, Supplementary Material The files of the interactive figure (192 images) of Figure 3, and the compressed (tar.gz) file of the 3 machine-readable table files (a portion shown for guidance regarding its form and content in Table 1) are archived on Zenodo. Figure 3. Top Panels: The hydrogen temperature profiles (left panels) along with the adiabatic prediction (red dashed line) in the CPI and NPI cases, and the line emissivities (right panels) of the superwind models on a logarithmic scale, from top to bottom, in the CPI and NPI cases. Bottom Panels: The hydrogen density profiles (left panels) along with the adiabatic prediction (red dashed lines), and the ionic fractions (right panels) on a logarithmic scale for the CPI and NPI cases. The start and end of the hot bubble (region b), the end of the shell (region c), and the Strömgren radius are shown by dotted, dashed, dash-dotted, and solid lines (gray color), respectively. Table 1. Integrated luminosities (unit in erg/s) from the different ionization models. Citation @article{Danehkar2021, author = {{Danehkar}, A. and {Oey}, M.~S. and {Gray}, W.~J.}, title = {Catastrophic Cooling in Superwinds. III. Nonequilibrium Photoionization}, journal = {ApJ, accepted}, volume = {937}, number = {2}, pages = {68}, year = {2022}, doi = {10.3847/1538-4357/ac8cec} } Learn More Website: https://superwinds.astro.lsa.umich.edu/ GitPage: https://galacticwinds.github.io/